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dc.contributor.authorWurster, J.
dc.contributor.authorBate, Matthew R.
dc.date.accessioned2019-10-25T10:30:03Z
dc.date.available2019-10-25T10:30:03Z
dc.date.issued2019-06
dc.identifier.citationWurster , J & Bate , M R 2019 , ' Disc formation and fragmentation using radiative non-ideal magnetohydrodynamics ' , Monthly Notices of the Royal Astronomical Society , vol. 486 , no. 2 , pp. 2587-2603 . https://doi.org/10.1093/mnras/stz1023en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 262150069
dc.identifier.otherPURE UUID: 73945391-99f8-41f8-a7e7-243655bf674e
dc.identifier.otherBibtex: WursterBate2019
dc.identifier.otherScopus: 85067995621
dc.identifier.otherORCID: /0000-0003-0688-5332/work/63716928
dc.identifier.urihttps://hdl.handle.net/10023/18767
dc.description.abstractWe investigate the formation and fragmentation of discs using a suite of 3D smoothed particle radiative magnetohydrodynamics simulations. Our models are initialized as 1 M⊙ rotating Bonnor–Ebert spheres that are threaded with a uniform magnetic field. We examine the effect of including ideal and non-ideal magnetic fields, the orientation and strength of the magnetic field, and the initial rotational rate. We follow the gravitational collapse and early evolution of each system until the final classification of the protostellar disc can be determined. Of our 105 models, 41 fragment, 21 form a spiral structure but do not fragment, and another 12 form smooth discs. Fragmentation is more likely to occur for faster initial rotation rates and weaker magnetic fields. For stronger magnetic field strengths, the inclusion of non-ideal MHD promotes disc formation, and several of these models fragment, whereas their ideal MHD counterparts do not. For the models that fragment, there is no correlation between our parameters and where or when the fragmentation occurs. Bipolar outflows are launched in only 17 models, and these models have strong magnetic fields that are initially parallel to the rotation axis. Counter-rotating envelopes form in four slowly rotating, strong-field models – including one ideal MHD model – indicating they form only in a small fraction of the parameter space investigated.
dc.format.extent17
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the final published version of the work, which was originally published at https://doi.org/10.1093/mnras/stz1023en
dc.subjectAccretion: accretion discsen
dc.subjectMagnetic fieldsen
dc.subjectMHDen
dc.subjectMethods: numericalen
dc.subjectPlanets and satellites: formationen
dc.subjectStars: formationen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleDisc formation and fragmentation using radiative non-ideal magnetohydrodynamicsen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1093/mnras/stz1023
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/1904.07263en


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